These mineral maps are derived using Multiband Imager (MI_MAP_02) reflectance data and Hapke radiative transfer modeling. These maps present the abundance of the four major lunar minerals (plagioclase, olivine, low-Ca pyroxene, high-Ca pyroxene) at a spatial resolution of ~62 m/pixel. Details about the methods can be found in Lemelin et al. (2015) and Lemelin et al. (2019). These maps suggest that at least 3 pixels, corresponding to approximately 11,500 m2, at the bottom of the Dawes crater match the mineral composition of the Apollo 17 norites studied by Cernok et al. (2021): 6-7 wt. % olivine, 47-52 wt. % orthopyroxene, 6-7 wt. % clinopyroxene and 35-41 wt. % plagioclase. Cernok et al. (2021) Sample-based evidence for an ancient (~4.2 Gyr) formation of the Serenitatis Basin on the Moon, Communications Earth & Environment (In press). Lemelin et al. (2015) Lunar central peak mineralogy and iron content using the Kaguya Multiband Imager: Reassessment of the compositional structure of the lunar crust, JGR - Planets, 120(5), 869-887. Lemelin et al. (2019) The compositions of the lunar crust and upper mantle: Spectral analysis of the inner rings of lunar impact basins, Planetary and Space Science, 165, 230-243.